adsabs/AstroCLIMB huggingface dataset:
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: The chi-squared values of the differences between the polarization angles observed by the JCMT and those predicted by the WK model as a function of inclination angle.
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: A map of radii of curvature in units of arcseconds. A radius of curvature is obtained using the observed polarization segments at 850 μm, as explained in the main text. The gray outlined pixels have radii of curvatures smaller than 36″. Most of these are located in the outskirts of the map.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: a) X-ray (2–10) keV intrinsic flux as a function of the [O IV] 25.9 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The open triangles show the uncorrected Compton-thick objects, while the filled triangles the corrected Compton-thick objects and the black dotted vertical lines show the applied correction. The solid line represents the linear regression fit with all objects, while the dashed line shows the fit to only Compton-thin objects (see Table 6). (b) X-ray (2–10) keV intrinsic luminosity vs. [O IV] line luminosity (both in logarithmic units of erg s−1). (c) Same as panel (a) but with the objects color coded: Seyfert type 1 (Sy1), blue; HBL region galaxies, magenta; Seyfert type 2 (Sy2), red; and LINERS (LIN), green. The solid line shows the fit for all Compton-thin type 1 AGNs, which includes both Seyfert 1s and HBL, while the dashed line gives the best fit for all type 2 objects, i.e., the pure Seyfert 2s, both Compton-thick and Compton-thin (see Table 6). (d) Same as panel (b) but with the objects color coded according to panel (c). The fits are similar to those in panel (c) but between luminosities (see Table 6).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [O IV] 25.9 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [O IV] line luminosity (both in logarithmic units of erg s−1). (c) Same as panel (a) but with the objects color coded: Seyfert type 1 (Sy1), blue; HBL region galaxies, magenta; Seyfert type 2 (Sy2), red; LINERS (LIN), green. (d) Same as panel (b) but with the objects color coded according to panel (c).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [Ne V] 14.3 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [Ne V] 14.3 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the [Ne V] 24.3 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. [Ne V] 24.3 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the [Ne V] 14.3 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. [Ne V] line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) [O III] 5007 Å line flux as a function of the [O IV] 25.9 μm line flux for all sources with reliable optical spectroscopic classification. Blue squares indicate Compton-thin objects, while red triangles are Compton-thick. The solid line shows the fit for all Compton-thin AGN, while the dashed line is the fit for all objects. (b) [O III] 5007 Å line luminosity vs. [O IV] line luminosity (both in logarithmic units of erg s−1). The solid line shows the fit for all Compton-thin AGN, while the dashed line shows the fit for all objects. (c) Same as panel (a) but with the objects color coded: Seyfert type 1 (Sy1), blue; HBL region galaxies, magenta; Seyfert type 2 (Sy2), red; LINERS (LIN), green. The solid line shows the fit for all Compton-thin type 1 AGN, which include both Seyfert 1s and HBL, while the dashed line gives the best fit for all type 2 objects, i.e., the pure Seyfert 2s, both Compton-thick and Compton-thin (see Table 7). (d) Same as panel (b) but with the objects color coded. All correlations are reported in Table 7.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) LED (Fernández-Ontiveros & Muñoz-Darias 2021) showing the Eddington ratio (in logarithmic form) as a function of the [Ne II]/[Ne II]+[O IV] line ratio, which measures the accretion disk dominance in an AGN, following the results of Fernández-Ontiveros & Muñoz-Darias (2021). The Eddington ratio has been computed using the bolometric luminosity as derived from the X-ray 2–10 keV luminosity. (b) Same as panel (a) but with the bolometric luminosity as derived from the [O IV] 25.89 μm line and the bolometric correction of Spinoglio et al. (1995) using the formula from Mordini et al. (2021).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) sSFR, i.e., sSFR = SFR/M ⋆, as derived from the [C II] 158 μm luminosities and the calibration of Mordini et al. (2021; see text) as a function of the specific BHAR, i.e., sBHAR = BHAR/M BH, as derived from the [O IV] 25.89 μm line luminosity and the calibration from Mordini et al. (2021), adopting the bolometric correction of Lusso et al. (2012) for all objects and only Compton-thin galaxies. Blue squares indicate Compton-thin objects, while red triangles are Compton-thick. The solid line shows the fit for all Compton-thin AGN, while the dashed line is the fit for all objects. (b) Same as panel (a) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies. The value of the correlations is given in Table 7. (c) Same as panel (a) but with the SFR as derived from the PAH 11.3 μm feature as measured from low-resolution Spitzer data (Wu et al. 2009) and the calibration from Xie & Ho (2019). (d) Same as panel (c) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) SFR derived from the [C II] 158 μm fine structure line as a function of the stellar mass of the galaxies. The galaxies are divided into Compton-thick and Compton-thin, and the given fits are indistinguishable. The dashed–dotted line represents the so-called main sequence for star-forming galaxies (Elbaz et al. 2011). (b) Same as panel (a) but with the color coded galaxy types. (c) Same as panel (a) but with the SFR derived from the PAH 11.25 μm emission band and the calibration from Xie & Ho (2019). (d) Same as panel (c) but with the color coded galaxy types.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) SFR as derived from the [C II] 158 μm line luminosity and the calibration of Mordini et al. (2021) as a function of the BHAR as derived from the [O IV] 25.89 μm line luminosity and the calibration from Mordini et al. (2021), adopting the bolometric correction of Lusso et al. (2012) for all objects and only Compton-thin galaxies. Blue squares indicate Compton-thin objects, while red triangles are Compton-thick. The solid line shows the fit for all Compton-thin AGN, while the dashed line is the fit for all objects. (b) Same as panel (a) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies. The value of the correlations is given in Table 7. (c) Same as panel (a) but with the SFR as derived from the PAH 11.3 μm feature as measured from low-resolution Spitzer data (Wu et al. 2009) and the calibration from Xie & Ho (2019). (d) Same as panel (c) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) Eddington ratio as a function of bolometric luminosity as derived from the X-ray 2–10 keV luminosity for the subsample of 12 μm AGN with a black hole mass estimate. Triangles indicate the Compton-thick sources, and the lines indicate three distinct black hole mass loci at 107, 108, and 109 M ⊙. A clear separation between the HBL and Sy2 populations is not observed in either the Eddington ratio or the bolometric luminosity. (b) Same as panel (a) but with the bolometric luminosity as derived from the IR [O IV] 25.9 μm line and the bolometric correction of Spinoglio et al. (1995) using the formula from Mordini et al. (2021).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) Bolometric luminosity as derived from the 2–10 keV X-ray luminosity using the Lusso et al. (2012) bolometric correction as a function of the bolometric luminosity as derived from the [O IV] 26 μm line luminosity and the bolometric correction of Spinoglio et al. (1995) according to the formula from Mordini et al. (2021). The luminosities are expressed in logarithmic units of 1041 erg s−1. (b) Same as panel (a) but with the objects color coded.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [Ne V] 24.3 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [Ne V] 24.3 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) AGN bolometric luminosity as a function of the [O IV] 25.89 μm line luminosity. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) AGN bolometric luminosity as a function of the [Ne V] 14.32 μm line luminosity. (c) AGN bolometric luminosity as a function of the [Ne V] 24.32 μm line luminosity.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic luminosity as a function of the [O IV] 25.9 μm line luminosity for all sources with a measure of the nuclear 12 μm luminosity. The blue squares indicate the AGN with L 12 μm > 1044 erg s−1, while red triangles show objects with L 12 μm < 1044 erg s−1. The solid line represents the linear regression fit with low-luminosity objects, while the dashed line shows the fit to the high-luminosity objects. (b) Same as panel (a) but with the AGN divided by their Eddington ratio. The blue squares indicate the AGN with ﹩\mathrm{log}({\lambda }_{\mathrm{Edd}})\gt -1.5﹩, while red triangles show objects with ﹩\mathrm{log}({\lambda }_{\mathrm{Edd}})\lt -1.5﹩.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [O III] 5007 Å line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [O III] 5007 Å line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the [O III] 5007 Å line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. [O III] 5007 Å line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [Ne III] 15.55 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [Ne III] 15.55 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the [Ne II] 12.81 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. [Ne II] 12.81 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the [Ne III] 15.55 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. [Ne III] 15.55 μm line luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the [Ne II] 12.81 μm line flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. [Ne II] 12.81 μm line luminosity (both in logarithmic units of erg s−1).